Hawking radiation is the detectable indicator of black hole evaporations. This work investigates the secondary spectra of particle radiation from black holes formed by the decay of directly emitted elementary particles into stable final products. Secondary spectra from both Schwarzschild and maximally rotating Kerr black holes are investigated. Spectra from black holes of masses between ~1013 g and Planck mass are considered in the present epoch within the context of the Standard Model. C code BlackHawk was used to simulate the emission spectra. The spectra consisted of photons, electrons, three types of neutrinos, and protons. A significant fraction of particles having energies below the black hole temperature was formed by the decay of unstable particles such as quarks, gluons, muons, tau, W±, Z0, and Higgs bosons. The elementary particles with high energies in the secondary spectra were predominantly the high energetic particles directly emitted by the black hole. The spectrum of protons from black holes beginning to emit coloured particles did not resemble the spectra of other secondary particles. As the temperature of the black hole was increased, the flux of protons increased. The decay products of directly emitted particles dominated the spectra at lower energies, but the spectra at higher energies were mostly comprised of directly emitted high energetic particles. There were significant differences between the spectrum from a Schwarzschild and maximally Kerr black hole beginning to emit coloured particles. Many oscillations were present in the high-energy end of the spectrum of Kerr black hole in contrast to the smooth variation observed from the same mass Schwarzschild black hole. The emission rates of protons were also higher in the Kerr black hole. However, the spectra from lower mass Kerr black holes were almost the same as the spectrum from the Schwarzschild black hole of similar mass.
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